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    Most High-density Exoplanets Are Unlikely to Be Remnant Giant Planet's Cores by Zifan Lin, Saverio Cambioni, Sara Seager

    Published 2025-01-01
    “…Upon envelope loss, the molten part of the planets can rapidly rebound owing to low viscosity, resulting in a decrease in radius by at most 0.06%, if they had hydrogen/helium envelopes, or by at most 7%, if they had H _2 O envelopes, compared to self-compressed counterparts with the same core mass fraction. …”
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    Revised Masses for Low-density Planets Orbiting the Disordered M-dwarf System TOI-1266 by Dakotah Tyler, Erik A. Petigura, James Rogers, Jack Lubin, Andreas Seifhart, Jacob L. Bean, Madison Brady, Rafael Luque

    Published 2025-01-01
    “…With bulk densities of ρ _b = 1.25 ± 0.21 g cm ^−3 and ρ _c = 1.51 ± 0.39 g cm ^−3 , the planets are among the lowest density sub-Neptunes orbiting an M dwarf. …”
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    Jupiter Evolutionary Models Incorporating Stably Stratified Regions by Roberto Tejada Arevalo, Ankan Sur, Yubo Su, Adam Burrows

    Published 2025-01-01
    “…We address the issue of which broad set of initial conditions for the planet Jupiter best matches the current presence of a “fuzzy core” of heavy elements, while at the same time comporting with measured parameters such as its effective temperature, atmospheric helium abundance, radius, and atmospheric metallicity. …”
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    Detectability of Emission from Exoplanet Outflows Calculated by pyTPCI, a New 1D Radiation-hydrodynamic Code by Riley Rosener, Michael Zhang, Jacob L. Bean

    Published 2025-01-01
    “…We show that the most detectable spectral lines tend to be the 589 nm Na i doublet and the 1083 nm metastable helium triplet. H α and Mg i 457 nm are moderately strong for some planets at some metallicities, but they are almost always optically thin, so some of their emission may not be from the outflow. …”
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    Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores by Ankan Sur, Roberto Tejada Arevalo, Yubo Su, Adam Burrows

    Published 2025-01-01
    “…With the recent realization that there likely are stably stratified regions in the interiors of both Jupiter and Saturn, we construct new nonadiabatic, inhomogeneous evolutionary models with the same microphysics for each that result at the present time in respectable fits for all major bulk observables for both planets. These include the effective temperature, radius, atmospheric heavy-element and helium abundances (including helium rain), and the lower-order gravity moments J _2 and J _4 . …”
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